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hi everyone

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um so my name is caprice phillips and my

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pronouns are she her and hers

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um i'm a phd student at the ohio state

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university working with dr

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g wong and today i'm going to be talking

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about

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the research that i've been working on

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involving detecting potential buyer

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signatures in the atmospheres of gas

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drawers with the james webb space

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before i get started i wanted to

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introduce my

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collaborators um so um my advisor is dr

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ji wong here

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at osu then we also have sarah kendrick

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the space

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telescope science institute who's an

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expert with mary

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we also have tom green who works at nasa

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ames who's a near spec

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expert in renew at jpl who does

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photochemical modeling and joel schultz

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and wendy panero

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who are both in the geology department

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and helpful

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with interior modeling and then jeff

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lenty at the space

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science telescope institute was also a

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new spec instrument so we've assembled a

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really great team

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of experts with different instruments

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with a board jwst

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it's been really great working with all

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um so gas dwarfs are among the most

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abundant type of planet so this is the

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type of planet that my research focuses

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on

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um and so in 2014 buchavi at all

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worked on a paper where they broke um

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exoplanets up into three categories

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based on

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solar metallicity and there were those

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be um below one point one point seven

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earth radii

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and above three point four right three

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but the ones in between um were dubbed

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uh

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gas droves which they said were rocky

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plant with

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planets with rocky cores and hydrogen

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helium

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envelopes and those include both super

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earths

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and many neptunes and so this is a

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diagram

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uh shown here it's a little outdated but

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it's the number of planets

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um versus the type of planets here and

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highlight are super earths and

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subneptunes showing that

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they're the most common type of

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transiting planet

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by size which is what my research

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focuses on

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um so what's interesting um about these

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types of planets is that they are not

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found

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in the solar system we have a very

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structured solar system

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where we have the inner rocky planets

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like mercury venus earth and mars

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we have gas giants like jupiter and

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saturn and then we also have

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ice giants um uranus and neptune and so

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gas dwarfs are not found in the solar

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system so

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it begs the question are they upscaled

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versions of the inner rocky planets are

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they downscaled versions

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of the gas giants for example and it

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brings forth questions about like the

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information

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atmosphere and if their bio signatures

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or potential signs of life

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are different in these types of planets

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um so ammonia is a biosignature so this

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was first

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proposed by sarah seeger in 2013

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and so the idea is that ammonia is a

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biosignature

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in an atmosphere rich in hydrogen and

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nitrogen

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the idea is that you might have

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microbial life that can break apart the

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bonds to produce ammonia

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and eventually we have an access to

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build up

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and the atmospheres are hopefully

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detectable levels and

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these microbial vibes can capture the

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energy release and the excess of ammonia

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like i said will build up in the

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atmosphere to

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potentially detectable levels and

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ammonia is a really

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cool biosignature in the potential buyer

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signature

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and the fact that you need really high

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temperatures and pressures to produce it

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a biotically so that's kind of the idea

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if you were to see

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potentially um detect among your

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atmosphere it could be the first steps

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to start to rule out abiotic

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processes and different things like that

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so my research focuses on if we can

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detect ammonia in the atmospheres of

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these gastro orbs

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so before we can even see whether we can

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detect ammonia we first have to

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select targets and so we'd use three

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main selection criteria and the first

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one

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we asked like kind of three questions

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like can the planet support liquid water

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um does the planet have the right

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pressure and third it's a planet

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um close enough to earth and so we want

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um it to have the right pressure between

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1.7

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and 3.4 earth radii and the uppercut

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is to make sure that it doesn't have too

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high repressor to produce ammo

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ammonia um abiotic it doesn't have a

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process

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like here on earth and so we want to

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make sure that the planet has the right

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temperature support

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and the water make sure it's not too hot

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and then also we want to make sure it's

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close enough

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um so that we have adequate flux from

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the whole star and the planet

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so based on this selection criteria

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we have a sample of seven targets shown

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on the right here

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that's the plot of the planet radius

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versus the equilibrium temperature

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of our seven targets we have targets

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like k2 18b

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lhs 1140b and a couple of planets in the

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toi 270 system

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so the targets are shown here in the

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color and the ones in the gray dots are

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the ones that meet

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the first two criteria but are more than

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um so we don't have the spectra for

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these

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um objects yet so what we have to do is

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have to simulate

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spectra and so what we

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we do that using this code called petite

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rate trans um developed by paul moliere

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in 2019 so it's a really cool program

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and that

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what you do is that you can insert an

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abundance of molecules you can edit the

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concentration

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of ammonia and different things like

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well water

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you can add rayleigh scattering

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different things like that and so you

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can also

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input pressure temperature profiles you

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can

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edit the surface gravity the size of the

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planet the temperature of the planet

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and where you want the pressure bar to

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be set at and if you would like to you

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can account for the effects of cloud

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decks as well and so on the right here

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is kind of is showing the example of the

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model outputs

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and so on the top here is showing

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um some kind of like new infrared like

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transmission

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spectroscopy of an example planet and on

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the bottom here is emission spectroscopy

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shown in the mid infrared

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to see whether we can detect ammonia

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features as well but these are the model

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outputs

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so um this slide encompasses basically

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the structure

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um of this research project so

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um the first step is um to build the um

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after we built the spectra we

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determine the amount of ammonia

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atmosphere and we start with

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a base amount of 4.0 um

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ppm in the atmosphere and also that's

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step one

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and so step two we select an instrument

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to test so

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there are a lot of ammonia features in

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the near infrared there's also

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a pretty dominant um ammonia feature in

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the mid-infrared and so we

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utilize different instruments to test

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whether we can detect

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these different features and so for the

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beginning at the top here we use

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the mirror instrument which is the

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mid-infrared

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instrument above aboard jwst

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which can there's around a 10 micron

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ammonia feature that we want to see if

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we can detect with emission spectroscopy

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and so we move on um select the

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instrument and then we also we vary the

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amount

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of hydrogen in the atmosphere and we

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either choose a 90

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hydrogen dominated atmosphere or 25

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hydrogen based atmosphere which changes

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the mean molecular weight of the

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atmosphere

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respectively and after that for mary we

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want to ask the question if we can

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determine

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if the ammonia features can be detected

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reacts as a contrast

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between the um planet and the stars are

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greater than equal to 10 to the

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minus four which is a sensitivity

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threshold for mary

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and so we kind of go back to step two

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with the near spec instrument which

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operates in the

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excuse me in the near infrared and so we

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go back in the x

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we vary again the amount of hydrogen in

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the atmosphere

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and so with a um 90 based hydrogen

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atmosphere we also

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want to detect we also want to see the

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effects that clouds have on the

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detectability and so we

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do clouds versus no clouds here and then

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for nearly with transmission

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spectroscopy

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we access a signal to noise for these

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ammonia features

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greater than equal to uh three sigma

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determine if that's a

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so we found that transmission

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spectroscopy is better

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suited to detect ammonia features than

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emission spectroscopy

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um so as i mentioned with transmission

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spectroscopy

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well we test a variety of instrument

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instruments and modes like the new spect

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and the nearest instrument is an example

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spectrum of toi 270 see here this is our

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simulated spectra

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from petite and the orange here and the

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black dots

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are the um simulated uh

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observations from jwst from the

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respective instruments shown down here

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at the bottom

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corresponding signal to noise for the

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different features

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um so if we take one feature among the

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future for example the 1.5

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among your feature here we see that with

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transmission spectroscopy we would get a

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signal to noise of 5 sigma which is

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great which would mean you would be able

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to detect this feature

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using that instrument for example um

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however when we go over to emission

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spectroscopy

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with mary as i mentioned before there's

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a ammonia future around 10 microns

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and we see that most of the targets here

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are below that sensitivity

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threshold for mary and even our best

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target lp79118c

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is barely above that

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sensitivity threshold so be very

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difficult to detect

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and so as we did this project we also

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wanted to

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test the effects that varying the amount

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of hydrogen

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and the atmosphere has for ammonia

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detection and we see that

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with a 90 hydrogen-based atmosphere for

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that same 1.5

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ammonia feature we have almost a double

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signal to noise value you go from a five

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sigma

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to a 25 percent hydrogen-based

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atmosphere to a two sigma

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detection um so we wanted to explore

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those effects and we see that it's

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better to have a higher concentration of

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hydrogen in the atmosphere to detect

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ammonia

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another thing we wanted to explore is

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the effects of clouds we see that

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clouds higher in the atmosphere cloud

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decks high in the atmosphere

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do kind of mute and fly in the

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transmissions

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spectra and so that's another effect

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that we wanted

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to see we tested a variety of cloud

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with that i'll just put up my conclusion

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slides

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and so we see that gastrops are more

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massive and common than earth

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and our promising sites look for signs

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of life and ammonia

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is an exotic biosignature unique to

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hydrogen-based atmospheres of gaf stores

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including super earth and many neptunes

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and we found that the near spec

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instrument is um

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better suited to mirror to detect

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ammonia than their specularized

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instrument

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and we exploit the effects of

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detectability of ammonia by seeing how

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it's affected by the concentration the

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atmosphere

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the amount of ammonia present in the

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presence of clouds